Converted to the Einstein frame, \(g^{\rm {\bf E}}_{\mu \nu }= e^{4\phi /(2-D)}g_{\mu \nu }\) , the \({D>2}\)  examples feature more severe curvature singularities and become geodesically incomplete e.g. [1]}, with singular deviations. \({D=2}\)  DFT is essentially Jackiw–Teitelboim gravity [2]}, [3]} as \(g^{\rm {\bf JT}}_{\mu \nu }= e^{-2\phi }g_{\mu \nu }\) . Witten's solution is then mapped to flat spacetime.
